Download chromospheric telescope of baikal astrophysical observatory. new light

Solar-Terrestrial Physics, 2016. Vol. 2. Iss. 2, pp. 82–103, DOI: 10.12737/21002. © INFRA-M Academic Publishing House
Original Russian version V.I. Skomorovsky, G.I. Kushtal, L.S. Lopteva et al., published in Solnechno-Zemnaya Fizika.
2016, vol. 2, iss. 2, pp. 69–85, DOI 10.12737/17376
CHROMOSPHERIC TELESCOPE OF BAIKAL ASTROPHYSICAL
OBSERVATORY. NEW LIGHT
V.I. Skomorovsky, G.I. Kushtal, L.S. Lopteva, V.A. Proshin, V.D. Trifonov, S.A. Chuprakov,
V.A. Khimich
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia, [email protected]
__________________________________________________________________________________
A chromospheric telescope is an important instrument for synoptic observations and solar research. After
several decades of observations with the chromospheric telescope at the Baikal Astrophysical
Observatory, a need arose to improve the characteristics of this telescope and filter. A new reimaging
lens to produce full-disk solar images 18 mm in diameter at the CCD camera Hamamatsu C-124
with a 36×24 mm detector (4000×2672 pixels) was designed and manufactured to replace the out-ofoperation 50×50 mm Princeton Instruments camera. A contrast interference blocking filter and new
calcite and quartz crystal plates were made and installed instead of damaged ones in the Hα birefringent
filter (BF), manufactured by Bernhard Hallе Nachfl. The optical immersion in the filter was changed. All
telescope optics was cleaned and adjusted. We describe for the first time the design features and their
related BF passband tuning. The wavefront interferograms of optical elements and telescope as a whole
show that the wavefront distortion of the optical path is within 0.25 λ. The BF and prefilter spectral
parameters provide high-contrast monochromatic images. Besides, we give examples of solar
chromospheric images in the Hα line core and wing.
Keywords: Solar telescope, birefringent filter, interferometric measurements.
_______________________________________________________________________________
INTRODUCTION
In 1980, SibIZMIR devised and manufactured the first domestic telescope for Нα filter observation
of the chromosphere of the full solar disk with spatial resolution of about 1″ [Banin et al., 1982].
Main parameters of the chromospheric telescope and filter
Diameter of the main lens
180 mm
Equivalent focal distance
5432 mm
Non-vignetted field of view
34 arcmin
Solar image diameter
50 mm
Birefringent filter, manufacturer
Bernhard Halle Nachfl. GmbH
Passband wavelength
λ 6563 Å
Passband half-width
1 or 0.5 Å
Passband shifts within
± 1 Å.
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V.I. Skomorovsky, G.I. Kushtal, L.S. Lopteva, V.A. Proshin, V.D. Trifonov, S.A. Chuprakov, V.A. Khimich
Over a period from 1981 to 1999, 50 mm solar images were taken using an 80 mm film. The film
archive is kept in the Institute of Solar-Terrestrial Physics SB RAS. In 2000–2002, the images were
captured by a Princeton Instruments CCD camera with a 50×50 mm matrix detector (2048×2048 pixels)
[ftp://ftp.iszf.irk.ru/h_alpha]. Since 2004, because of the camera failure, the images were obtained
manually with a Konica Minolta DiMAGE A2 8MP Digital Camera (3264×2448 pixels). The small camera
view (about 17 mm) allowed us to observe only individual active regions. To take full-disk images by a new
automatic Hamamatsu С9300-124 CCD camera with a 36×24 mm detector (4000×2672 pixels), we
temporally installed a commercial lens that produced 18 mm solar images. However, it did not provide
high-quality images; hence the need for a new reimaging lens. Moreover, in images there emerged areas
with different center-to-limb brightness, whose sharp jump pointed to instrumental origin, as well as dark
points in the field of view and drop-shaped defects at the field edge. They had been caused by defects
arising in the optical stack of the birefringent filter (BF) and in the prefilter. To correct the defects, we
had to repair and change BF polarization elements. Despite the relatively clean Baikal atmosphere, the
telescope optics over the 35-year period of year-round operation were covered with dust from the nearest
buildings under construction and with soot from forest fires. We had to completely dissemble, clean the
teleobjective and other optics of the telescope, and readjust the entire telescope.
DESCRIPTION OF THE TELESCOPE
The telescope and its optical scheme are shown in Figure 1. One of the conditions for successful operation
of the telescope – filter complex was the compliance of its optical scheme for image construction with BF
installation requirements largely in order to maintain the emission monochromaticity, specified by BF
parameters, and to provide the required resolution over the entire solar disk.
Particular original design solutions for optical elements and some other essential unites of the
chromospheric H telescope are presented in [Klevtsov, Trifonov, 1980].
BF – the most important element of the chromospheric telescope – is a unique instrument that costs
as much or even more than the telescope. The clear aperture of the BF optical stack is 28 mm; the length,
190 mm; the filter field of view, ±2.5° with allowable passband shift of 0.05 Å. These parameters
suppress appetite for installation of the filter into a large aperture telescope for full-disk observation with
the highest, less than 1′′, resolution [Klevtsov, 1984]. It was just this filter for which we calculated the
optical scheme and manufactured the telescope to capture full-disk monochromatic solar images at spatial
resolution of about 1 with allowance made for resolution characteristics of emission receivers (motion
picture films, CCD matrix).
83
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
F
Figure 1. Chrom
mospheric telescope of the Baiikal Astrophysical Observatory
y and its optical
al scheme
W
We did not taake on an inv
verse task to work out a filter for the finished teleescope: in 197
70-80s
manufactures sougght to design BF
B with extreeme characterristics determined by curreently availablee filter
matic solutionss, birefringentt crystals, andd by processing and control capabilities. L
Large homogeeneous
schem
calcitee crystals requuired for largee aperture filteers are rare in nature and if available it is unreasonablee to cut
them for a medium
m-quality filterr. The crystalss may be kept in reserve unttil new schem
mes and techno
ologies
have bbeen developeed.
A
An interferencce filter (IF), a prefilter com
mprised of a metal
m
– dielectrric – metal (M
MDM) heat filtter and
a narrrowband interfference filter, transmits lighht only in a naarrow spectral region with a central waveelength
and rreflects all the emission back through the telescopee lens. Inside illuminationn of lenses by
y light
refleccted from the filter
f
balancess the outside hheat flux and decreases
d
temp
perature gradiients in lenses.
B
Before the “fi
first light” of the chromosppheric telesco
ope, we exam
mined spectrall characteristiccs and
waveffront of BF annd IF. Spectral characteristiccs of BAO BF were similar to those reporrted for the Beernhard
Halle filter of the Sayan
S
Solar Observatory
O
[S
Skomorovsky, 1967]. In the crystal stackk and BAO BF,
B we
T
were dim
minished by a special laborratory-processsed transparen
nt plate
revealled wavefrontt distortions. They
that hhad been opticcally polished
d and retoucheed to compen
nsate these disstortions. Thee plate was in
nstalled
outsidde of the BF crrystal stack.
T
Teleobjective and
a field lens. The calculattion of the opttical scheme and the choicee of lens design
n were
limiteed to the use of
o a long focall-length lens: the telescope should be no
o more than 4 m long to fit within
the paavilion dome. The short length of the oobjective unit of the telesco
ope is due to the two-comp
ponent
teleobbjective. A priincipally new idea was to in
install the field
d lens in front of the primaary image to shorten
s
the telescope tube [Banin et al., 1983а]. The focal distancee of the field lens is equal to its distance from
mage of pupil created by thee negative com
mponent of th
he lens. The field lens transffers the pupil image
the im
to inffinity and form
ms in the mid
ddle of the fillter an interm
mediate solar image
i
20 mm
m in diameter in the
teleceentric beam paath. This proviides homogenneous spectral composition of all image ppoints.
T
The telescope is designed to
o produce a hiigh-quality im
mage in the foccal plane onlyy in one wavellength;
and thhis beneficiall feature enab
bles us to usee for the teleeobjective onlly two singlee-lens (uncem
mented)
84
V.I. Skomorovsky, G.I. Kushtal, L.S. Lopteva, V.A. Proshin, V.D. Trifonov, S.A. Chuprakov, V.A. Khimich
components, positive and negative, making them from one material and with radii of curvature that are
equal in size but different in sign. The latter is very favorable for the mutual control of radii of curvature
and lens surface shape when manufactured.
The lens reconstructs and enlarges a solar image so as not to lose the resolution expected of the
telescope on film and then on matrix. If we accept that the actual resolution of film coating with relatively
high resolution of 200 line/mm for low-contrast chromospheric structures is 30 line/mm, a solar image
should be no less than 50 mm. This roughly corresponds to the resolution of 1.3″.
In the telescope scheme, the problems of control and adjustment have been successfully solved: the
main lens and zooming lens were corrected for spherical aberration, thus providing independent control of
each component in the autocollimation scheme with a plane mirror. We virtually eliminated the entire
telescope system from spherical aberration, coma, and astigmatism. The tolerances for radii, thicknesses,
inter-lens distances, and refractive indices of lenses are quite low. High tolerances exist for decentration
of teleobjective, i.e. for wedge, rotation, and displacement of the lenses perpendicular to the optical axis
[Klevtsov, Trifonov, 1980]. Adjustment of lenses in the telescope (tilt, displacement of lenses) was
controlled using interference images in the lenses with the aid of a laser. The wavefront of the
teleobjective and telescope after the first assembly with the filter optical stack simulator, which was
installed instead of BF and transmitted laser light, was tested in the autocollimation scheme. Figure 2
shows wavefront interferograms of the teleobjective and telescope.
Observational materials on the solar chromosphere obtained with the telescope, their processing and
interpretation are reported in research papers and theses by ISTP SB RAS and other researchers [Banin et al.,
1983b; Banin et al., 1986; Borovik, Myachin, 2002, 2010; Golovko et al., 2002; Batmunkh et al., 2011;
Borovik et al., 2014; Konyayev et al., 2015].
MODERNIZATION OF THE TELESCOPE IN 2015
Since the CCD camera was changed to another one with a matrix half as large, we had to calculate
and make a new reimaging lens because the temporary commercial lens in use did not produce a highquality image. Fading of film coatings of the MDM heat filter, installed before BF, in the solar beam
caused image brightness to vary across the field of view. It was immediately obvious that this was due to
inhomogeneity of the prefilter passband.
In addition, we discovered defects in BF polarization elements – cement defects and cracks. The
chromospheric telescope operating for many years, its optics was brought out of center, the filter appeared
to be displaced, and edge defects of its optical stack also appeared within the field of view.
85
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
F
Figure 2. Waveefront interferogram of the telleobjective and
d telescope [Klevtsov, 1987]. The wavefrontt of the
telescoope is close to the
t theoretical limit
BIREFRINGENT FILTER
T
The company Bernhard Hallle (West Berl
rlin) has produ
uced about 20
00 Lyot-Ohmaan filters [Bhaatnagar,
Livinggston, 2005]. In 1960s, Asttrocouncil of tthe USSR Accademy of Sciiences received
ed ten Нα filteers and
distribbuted them am
mong USSR ob
bservatories: IZ
ZMIRAN and SibIZMIR obsservatories, Crrimean Astroph
hysical
Obserrvatory (AO), Mountain
M
Stattion of the Cenntral Astronom
mical Observattory, Ussuriyskk AO, Tashkent AO,
and U
Ukraine MAO
O in Goloseyeevo. Studies oof B. Halle filters
fi
[Skomorrovsky, 1967]] revealed thaat their
transm
mittance was not
n less than 10
0 % because thhe scheme invo
olved split polaarization stagees [Evans, 1949
9] with
a smaaller number off polarizers thaan in the classsical scheme. The
T filters had a narrow, aroound 0.5 Å, paassband
and hhigh contrast (the
(
relation between transm
mittance in fallse peaks and main peak) ddue to the add
ditional
repeatted polarizationn stage introdu
uced into the sscheme [Öhmaan, 1958]. Sollar telescopes pproduced fairly good
imagees with Нα filters. All these filters had alm
most identical life
l history: po
olarizers faded owing to inad
dequate
protecction of filter optical
o
stack fro
om solar radiattion.
O
Of particular innterest is the history
h
of the first B. Halle filter, receiveed by SibIZMIIR in 1961, th
hat was
emplooyed for year-round observaation performeed at the Sayaan Solar Obseervatory. In heeavy frost, thee diesel
powerr station failedd, the filter waas not put awayy into a warm
m place in timee, and there em
merged defectss in the
opticaal stack. Opticcal enterprises could not reppair the filter. And only A..B. Gilvarg, thhe optician fro
om the
Instituute of Crystalllography, Russsian Academyy of Sciencess, a creator off the first dom
mestic BF [Seeverny,
Gilvarrg, 1949], helpped to test the filter. It appeaared that the op
ptical stack consisting of neaarly 60 elemen
nts was
cemennted with Cannada balsam. In
I thermostat, at high tempeerature, at the risk of overhheating/damagiing the
polarizzers, the stack was disassemb
bled and defeccts were found: calcite crystaal plates were ccracked.
W
With a desire to repair the unique instrum
ment ourselvees, we began to search for crystals and to
t gain
familiiarity with opptical technolo
ogy. We deveeloped precisio
on methods fo
or processing and controlliing BF
crystaal plates [Kusshtal, Skomoro
ovsky, 2002],, reconstructeed the out-of-o
operation B. H
Halle Нα filteer, and
workeed out new BFs
B [Aleksand
drovich et al., 1975; Kushtal, Skomorov
vsky, 2000]. In actual fact, all B.
Halle filters of the USSR solar observatories
o
w
were repaired and got “seco
ond and third light” at the Optical
O
I
Laborratory of our Institute.
86
V.I. Skomorovsky, G.I. Kushtal, L.S. Lopteva, V.A. Proshin, V.D. Trifonov, S.A. Chuprakov, V.A. Khimich
Into the chromospheric telescope of the Baikal Astrophysical Observatory, we put a B. Halle Нα filter of
younger, 1968, generation. Until 1980, it worked at the Horizontal Solar Telescope. Such filters are still
exploited at many observatories. We utilize the BAO filter to describe the method adopted to tune the filter,
present the optical scheme, main blocks, and kinematics of the filter (Figures 3, 5). Features of certain elements
and stages of the optical stack of this filter as well as schemes of filters known at that time are described in
[Skomorovsky, Ioffe, 1980].
In B. Halle filters of this generation, optical stack elements, except for film polarizers cemented
between glasses, were assembled by immersion. This facilitated disassembly of the optical stack. Over the
35-year period of the B. Halle filter operation at the chromospheric telescope, BF has been repaired at
BAO several times: we removed the blocking of the line-shifter mechanism, changed the prefilter fading
owing to the heating in a beam as well as the external polarizer and polarizers inside the optical stack,
which gradually faded owing to solar radiation. We established that immersion by which the crystal
elements were assembled could contact with the cement layer of old or newly installed film polarizers. It
gradually penetrated along the perimeter between protective glasses, producing cement defects and
turbidity in the polarizers. The complete disassembly of the optical stack to replace the polarizers
necessitated the production of new quarter-wave phase plates for the line-shifter because they had been
made not from quartz but from crystalline mica (3, 11, 41, Figure 3). The very soft mica plates broke
down when disassembled and cleaned, and needed replacing. It was found out that the wavefront
distortions discovered in the filter and corrected by a retouched plate in "first light" were caused by the
deformation of thin glass plates (2, 12, and 42, Figure 3) installed outside of the optical stack to protect
the mica quarter-wave plates. We replaced these plates as well as calcite plates damaged by severe
overheating of the filter owing to the out-of-order thermoregulator.
Manufacturing BF crystal plates is a process in which during optical polishing it is necessary to ensure
pinpoint accuracy of thickness of the plate, parallelism and flatness of its surface. For the Iceland spar, the
production tolerance is 0.05 µm for each parameter. Figure 4 shows opticians at work. Not every highlyqualified optician can make new calcite plates by hand with the required tolerance.
We have manufactured a new crystalline quartz plate 1.6 mm wide with edge digs within the field of
view. We knew about the defect (the B. Halle company had an insufficient number of good crystals) but
did not change the quartz plate because the digs were out of a solar image.
By now, all external cemented polarizers have been changed to immersion-neutral polaroid films
without protective glasses. As a result, the optical stack became shorter by 20 mm. The filter optical stack
was cleaned of black dots (dust), reassembled, and “pumped” in immersion in vacuum to remove air bells
(cement defects) from the field of view. The immersion-reflection index (nd=1.578) is close to mean
crystal-reflection indices for ordinary and extraordinary beams. Immersion reduces light losses due to
Fresnel reflection by crystals and polarizers and compensates wavefront distortions caused by imperfect
surfaces of the stack plates numbering more than 100 in the filter (Figure 3)!
87
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
F
Figure 3. The optical
o
scheme of the B. Hallee Нα-filter crysttal stack. Thick
knesses of polar
arization split ellements
(III–IV
V stages) are not
n multiples of
o 2 because thhey contain haalf-wave and quarter-wave addditions. Stagess I–VII
comprrise polarizers and
a plates betweeen them
F
Figure 4. Opticiaans Khimich V.A
A. and Ivanov A
A.A. in the coursse of making plates for BF. In thhe right bottom corner
c
is
a plate damaged by ovverheating in BF. The wavy line of rupture indiccates the nonunifform heating (theermal shock)
T
This filter hass eleven classical BF polarrizer – crystal plate – polarrizer blocks coombined into seven
polariization stages four of whicch are split too reduce the number of po
olarizers. Threee stages, I, II,
I VII
(Figurre 3), made frrom Iceland spar,
s
are widee-angle, Lio I type, regular.. Four stages,, III, IV, V, VI
V with
calcitee and quartz plates are spllit, wide-anglle (except forr VI), Evans type.
t
The pollarization stag
ges are
locateed in two busshings (Figuree 5). A short bbushing featu
ures only two polarization stages I and II (see
Figuree 3). Stage II forms a 1 Å passband; annd stage I, thee so-called co
ontrast stage, aacts virtually as the
stage with a full width
w
at half maximum
m
(FW
WHM) of 1 Å.
Å The contraast stage becoomes effectivee if we
gnations in Fig
gure 3) on thee lever in the flange
includde in the stackk its external polarizer 1 (ssee also desig
“Сonttrast” (Figure 5) of the filterr housing (thee lever is moved from «Auss» to «Ein»). IIn the optical stacks,
s
88
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
b
F
Figure 5. Barrell of the filter crrystal stack (a); movable elemeents (b)
both eends of the shhort bushing have
h
quarter-w
wave plates 3 and 11; therefore we can sshift the passb
band of
both tthe stages by rotating
r
the bu
ushing aroundd fixed externaal polarizers.
A long, fixed bushing consiists of five (IIII–VII) polarizzation stages. On the side oof the short bu
ushing,
it has polarizer 13 of
o stage III. On
O the oppositte side is quarrter-wave platee 41 of stage V
VII with an FWHM
F
e
and tunable with external polaarizer 43 locaated on the leever of
of 0.55 Å. This stagge becomes effective
flangee 0.5 Å. The lever
l
is moveed from «1 Å»» to «0.5 Å» position.
p
The passband in aall the three tunable
filter stages is shifted from the general bushingg (line-shifterr, Figure 5) thrrough convenntional transmiissions
by rootating the short bushing around
a
fixed polarizers 1, 13 and by synchronous
s
rrotation of ex
xternal
polariizer 43 aroundd quarter-wav
ve plate 41 of the fixed stag
ge with the 0.5 Å FWHM iin the long bu
ushing.
The shhort bushing and
a external polarizer
p
43 arre conventionaally hooked with
w the 1:2 traansmission rattio.
STMENT OF
F THE BF P
PASSBAND
D
ADJUS
T
The goal of thhe adjustment is to match ppassbands of tunable
t
stagess, with the passsband of unttunable
stagess, and with the Нα line at operating
o
tempperature. An inaccurate
i
maatching of thee passbands caauses a
decreaase in transmiission and an increase
i
in seccondary peakss.
D
During adjustm
ment at the spectrograph, we should reducee the effect of such
s
a factor ass light polarizaation in
the spectrograph andd illumination system lenses upon the accu
uracy of stage matching.
m
Thee filter flange with
w the
unable stages should be direccted to the lam
mp; and the flaange with the 0.5 Å stage with
w the
contraast and 1 Å tun
turnedd-out external polarizer, to th
he spectrograpph slit. First, we
w match the passband
p
of thhe 1 Å stage with
w the
filter ppassband by rootating the sho
ort bushing with
th its turned-ou
ut polarizer. Yeet on the specttrograph slit we
w put a
depolaarizer to neutraalize the disturrbing light moddulation from the 0.5 Å stag
ge. Then, we addjust the contrast and
0.5 Å stages for maaximum transm
mission by tunning their own operating polaarizers. It is veery useful to employ
e
mission of theese stages, ussing not maxiimum but min
nimum
first tthe additional polarizers to adjust transm
transm
mission and symmetry
s
of secondary peaaks. This adju
ustment is more
m
accurate. Then, the working
w
polarizzers are simplly set to crosssed position w
with the additio
onal ones. Aftter having mat
atched the stag
ges, we
correcct the operatingg temperature of
o the filter to aaccurately adju
ust the passban
nd to the hydroogen line.
89
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
PROFIILES OF TH
HE BF AND
D INTERFER
RENCE PR
REFILTER P
PASSBAND
DS
S
Spectral characcteristics of BF
B were foundd at the laboraatory autocolliimating spectrrograph (F=6 m, the
apertuure ratio 1:30,, the grating 200×300
2
mm,, 600 groove//mm). The spectrograph annd its equipmeent are
detaileed in [Skomorrovsky et al., 2015].
2
The filtter was set in the
t parallel beam; spectra w
were registered by the
CCD linear array MORS.
M
Figure 6 illustrates sppectra of the paassband at 0, ±0.25,
±
±0.50, aand ±0.75 Å frrom the
Нα linne center. Furthher shift of thee passband leadds to a consideerable increasee in a secondary
ry peak becausse other
filter sstages are untuunable. Within the ±0.5 Å shiift, false peaks are low, and the passband ha
has a high contrrast.
IIn 1989 (befoore the curren
nt repair), foor preliminary
y monochrom
matization in B
BF we installed an
interfe
ference MDM heat filter and
d a narrowbannd dielectric in
nterference fillter. Coatings of these filterrs were
in vaccuum therefoore they weree well protectted from moisture [Prosh
hin, Aleksanddrovich, 1982
2], but
silverr layers were damaged by
y solar radiattion. In the photograph
p
(F
Figure 7, top right), this can
c be
seen iin the centrall part of the MDM
M
filter ((a reflection glare). The MDM-filter
M
trransmittance in the
centerr became tw
wo times less than at thhe edge. Botth the filterss have a go od wavefron
nt (for
transm
mission), butt, because they were seealed in vaccuum, their glasses weree deformed under
atmosspheric pressuure. The filteers must not be cemented together – th
hey should bbe installed in
nto the
opticaal stack with ann air gap betw
ween them to leeave the waveefront unaltered
d. Re-reflectioons in the air gap
g can
cause reflection glarres and false suns
s
in an imaage owing to obliquity
o
of BF
F. The sensitivvity area of thee CCD
camerra extends fartther than 1.1 µm, thereforee we supplemeented the tand
dem MDM-filtter+IF with a color
glass light filter SZ
ZS-25. Figuree 8 shows thee passband off the IF tandeem in the main
in peak in 198
89 (1),
its abbsorption in a broad spectrral region (2)), and absorption of the SZ
ZS-25 filter ((3) that comp
pletely
eliminnated secondary peaks at a distance off more than 0.9
0 µm, thus increasing
i
thee optical density of
the taandem from 2 to 6. The tottal transmittannce of the asssembly is nott given in the figure.
F
Figure 6. BF paassbands for 0, ±0.25, ± 0.5, annd ±0.75 Å possitions from thee Нα line centerr. They are norm
malized
relativve to the passbaand in zero possition. Filter traansmittance at zero position of
o the line-shiftter. Profiles forr all the
positioons are scaled up
u to distinguish
h the false peakks. As the passb
band shifts, the intensity Ic of th
the main peak reduces.
The FW
WHM decreasees from 0.43 Å at 0.25 Å to 0.339 Å at 0.75 Å
90
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
F
Figure 7. On thee right are prefiltters of 1989 (at the top) and 2015 (at the bottom
m). On the left iis the transmitttance of
the MD
DM filter in thee center (1) and
d on edges (2, 3))
T
The new prefiilter developeed in 2015 is comprised off three dielectrric filters: a nnarrowband co
ontrast
one w
with an FWHM
M of ~30 Å, an
nd two filters cutting up to 1.4 µm. Nineteen-layer cutt filters are deesigned
as 1/22λHLH…19....HL1/2λH with
w
H and L being mateerials with high
h
and low
w refractive indices
i
respecctively. Yet external
e
coatin
ngs are half-w
wave, made from ZnSe with
w a high reeflective index; and
internnal coatings arre quarter-wav
ve, applied altternatively by materials with high (ZnSe)) and low (Naa3AlF6)
refracctive indices. The multilayer filter coatiings are sealeed by optical cement. All the three filteers are
cemennted together and set in the barrel (the boottom photogrraph on the lefft of Figure 7)). Figure 8 illu
ustrates
the paassband of thhe narrowband
d IF (4), the IF optical deensity with on
ne cut filter ((5), and the optical
o
densitty of the IF asssembly with two
t cut filterss (6).
A
At 22 °С, the narrowband filter is centerred on λ 6581 Å, the transsmittance is 669 %; and in the
t Нα
line, tthe transmittannce is ~30 %. This filter wiith the 30 Å FWHM well su
uppresses secoondary peaks of BF.
Althoough the prefiilter is not ceentered on thee hydrogen liine, there is enough light,, transmitted by the
F system, to capture
c
imagess by the new ccamera with exposure time of several millliseconds.
IF+BF
REIMA
AGING LEN
NS
T
The primary soolar image 20 mm
m in diameteer is produced by the teleobjective and field
ld lens approxiimately
in the middle of BF. The new fou
ur-lens objectivve (Figure 9) trransfers the im
mage to the Ham
amamatsu С9300-124
x size is 24×366 mm; the imaage diameter, 18
1 mm. The obbjective also corrects
c
digitall camera (Japaan). The matrix
aberraations of prior optics. Since the
t laboratory had a limited set of radius operating
o
test gglasses, the ob
bjective
was caalculated as a two-componen
t
nt system. Eachh of the compo
onents includeed two lenses (ccrown, flint) with
w the
use off only two nom
minals of radii of
o curvature.
W
When the lensses were being
g treated, the interference control
c
of the shape of theirr surfaces wass made
with tthe operating test glasses; and
a the controol of centerin
ng, by measuring thickness of the lensess along
the eddge on a rotatiing table (Figu
ure 10) with thhe aid of an in
ndicator.
91
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
F
Figure 8. Spectraa of prefilter tran
nsmissions obtaiined by the Hitaachi U-3400 specctrophotometer. Along the X-ax
xis is the
waveleength in nanomeeters; along the Y-axis,
Y
the transm
mittance in % (1
1, 4), and the opttical density in aabsorption (2, 3, 5, 6)
F
Figure 9. Reim
maging lens (F=
=230 mm, D=700 mm) in the barrel:
b
1, 3 are positive
p
lenses ; 2 is a meniscus; 4 is
a magnnetic-base neggative lens
b
F
Figure 10. Tablle for measuring
g wedging of leenses (a); pressiing scheme (b)
92
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
B
Before measuuring lens thiickness, we sshould press the lens to th
he support off the rotating
g table
and seet it (with thee same indicaator) in such a way as to prrevent its ecccentricity wheen the table ro
otates.
A shoortcoming off most well-known table ddesigns is thaat the radial pusher
p
lever not only shiffts but
also ccan slightly raaise a lens, th
hus introducinng an error in
nto the contro
ol of its thickkness along th
he lens
edge. To improve thhe control accu
uracy, we workked out a new pendulous
p
desiign for the push
sher. The push
her side
bearinng up against the edge of the
t lens is bevveled and rou
unded; the rev
verse side is m
made in the fo
orm of
evolvent along whiich an adjustiing screw durring rotation slides
s
and moves the pusheer. The pusher itself
way on a spinndle, located below the adjjusting screw. When rotatiing, the screw
w presses the pusher
can sw
alwayys at right anggles to the ev
volvent, and tthe pusher, displacing
d
the lens lengthw
wise, simultan
neously
pressees it to the suppport of the ro
otating table.
E
Each componeent of the reim
maging lens iss assembled by
b immersion with a refracttive index nd=1.578.
=
The iinterference quality
q
control of the lenns was run with an uneequal-arm intterferometer in the
autocoollimation schheme (Figure 11) in the besst image planee.
F
Figure 12 shoows a calculated wave diffeerence of the beam path in the four-lenss reimaging leens for
an axxial point (a) and a wavefrront interferoggram in the double
d
beam path through the lens (b). Wave
aberraations of the reimaging lenss are close to eestimated ones and range within
w
0.1λ.
ASSEM
MBLY AND ADJUSTM
MENT OF TH
HE TELEO
OBJECTIVE
E
IN THE
E STANDAR
RD BARRE
EL
O
Over the 35--year period of operationn, the teleobj
bjective becam
me dirty andd needed com
mplete
disasssembly, cleaniing, and readju
ustment.
T
The standard barrel of the teleobjective is a tube abo
out 400 mm long
l
(Figures 13, 14). It feeatures
adjusttable tilt of thhe negative len
ns on the balll support of th
he back tube flange and addjustable leng
gthwise
displaacement of thiis lens relativee to the positivve lens, fixed motionlessly on the front tu
tube flange. There is
no meechanism for lens displaceement perpenddicular to thee optical axis because exacct centering of
o lens
barrells in the tube of the teleobjective and lennses themselves is specified
d by their desiign. The instaallation
of pulller bolts to thhe back flangee of the teleobbjective tube has
h proved useful in practicce. They can help
h to
removve the blockinng of the negative lens barreel with the len
ns tilt being ad
djusted on thee ball support. In the
tube ssidewall theree is a port thro
ough which w
we can put a baffler
b
to elim
minate secondaary reflection glares
duringg lens adjustm
ment.
F
Figure 11. Conttrol scheme in the
t best image pplane
93
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
b
F
Figure 12. Wavvefront of the leens for an axiall point: a is a computed
c
wavefront, Px, Py are
re radii of the entrance
pupil iin meridional annd sagittal plan
nes; b is a waveffront interferog
gram (double paath), λ 6328 Å
T
The teleobjecttive lenses aree installed intoo their barrels 1, 4 (Figure 13)
1 on three siide spacers plaaced at
an anggle of 120°. To
T the same barrels
b
during the lens adjustment, we fasten diaphraggms 7, 9 (FIgu
ure 13)
with aapertures 1–2 mm.
T
These aperturees are used to center a beam
m of the laser, installed togeether with screeen 5, on the side of
the poositive lens att a distance off ~1 m (Figurres 13, 15). Th
he beam tracees the positionn of the geom
metrical
axis oof the teleobjeective tube. Th
he positive lenns is nonadjusstable. It is sett perpendiculaar to the opticcal axis
by tiltting and transvversely displaacing the wholle tube by optiical bench meechanisms.
F
Figure 13. Adjjustment and control
c
of the tteleobjective in the barrel: 1 is the externaal tube (positiv
ve lens
barrel)); 2 is the inteernal tube with
h a ball supporrt; 3 is the adjjustment of inter-lens distannce; 4 is the neegative
lens b arrel; 5 is the laser with the screen; 6 is thhe reference flaat mirror; 7 is a diaphragm; 8 are the adjusstments
phragm; 10 is tthe unequal-arm
m interferometter
of the negative-lens tilt; 9 is a diap
94
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
F
Figure 14. Deviice with the flatt etalon and inteerferometer to control
c
the wav
vefront of the teeleobjective
F
Figure 15. The laser with the screen
s
b
a
c
F
Figure 16. Appeearance of an in
nterference imagge during match
hing of reflectio
on glares. Refleection glares only from
the possitive lens are seeparated (a), coincide (b). Refleection glares fro
om four surfaces of the two lensses coincide (c)
T
The control iss implemented
d on the screeen, using refleection glares reflected
r
from the lens surfface. A
reflecction glare froom its front convex
c
surfacce is blurred; that from itss back concavve surface, fo
ocused
(Figurre 16, a). As reflection glaares approachh each other, we observe an
a interferencee ring image that is
centerred at the screeen aperture by
y tilting the lenns (tube) (Figurre 16, b). Refleection glares frrom the negative lens
can bee temporarily blocked
b
with a baffler lest thhey impede. Nevertheless, we should contrrol beam propaagation
througgh apertures off the diaphragm
ms of both the lenses and, if necessity,
n
correect the laser’s pposition.
A
After adjustmeent with reflecction glares frrom the positiv
ve lens, we firmly fix the te
teleobjective tu
ube on
the opptical bench. Reflection glares from thee negative len
ns are also ceentered at thee screen aperture by
adjustting the tilt off the barrel on the ball suppoort before the interference im
mage appears within this leens and
95
Chromospheric telescope of Baikal Astrophysical Observatory. New light
between lenses. When reflection glares from the lenses are situated near the screen aperture, they are
precisely centered at the aperture by tilting the lenses; and interference images are displaced and centered by
parallel displacement of the lenses. If centers of three images cannot be matched by changing the negativelens tilt, it is necessary to displace the lens in the barrel toward matching of the images by changing spacers.
The screen (Figure 16, c) exhibits three systems of Newton interference rings: two from the lenses and one,
wider, from surfaces of the air gap. The latter reacts to vibrations in a building and air turbulence in it. With
required tolerances for centering of the lens, the admissible spacing between image centers is no more
than 0.5 mm at a distance of 2 m from the lens to the screen [Klevtsov, 1987].
STUDYING THE WAVEFRONT OF THE TELEOBJECTIVE
In focus of the teleobjective, we set unequal-arm interferometer 10 (see Figures 13, 14) centered at the
same apertures of the diaphragms on barrels of the teleobjective lenses; and on the side of the positive lens, we
install reference flat mirror 6 to control the wavefront in the autocollimation scheme. Note that the teleobjective
was adjusted using special laser 5 instead of interferometer laser 10 (Figure 13) because in the beam splitting
cube of the interferometer there occurred additional reflection glares impeding the adjustment.
Wavefront interferograms in the double beam path were obtained for a point on the axis of the
teleobjective with a distance of 345.5 mm between the lenses. With this distance, the teleobjective – field
lens system produces an intermediate solar image in the middle of the BF optical stack. Figure 17 shows
interferograms obtained in 2015 before disassembly (b) and after cleaning and assembly (c). For
comparison, we give the previously presented wavefront interferogram (Figure 2) of the lens after the first
assembly in 1980 (Figure 17, a). Below are calculated wavefront profiles for axial points and at a distance
of 16 arcmin (d).
Over the 35-year period of the telescope operation, the adjustment and wavefront of the teleobjective
have changed little, if at all. The newly adjusted lens shows the wavefront not worse than before
disassembly, and even closer to the calculated value. Differences between interferograms can be caused
by airflows in the building and by temperature gradients on the lenses that appear despite air blowing of
the control zone.
ADJUSTMENT OF THE WHOLE OPTICAL SYSTEM
OF THE CHROMOSPHERIC TELESCOPE
On the optical bench, we set the telescope tube without optics (Figure 18) assembled from the
following blocks: teleobjective flange 1, declination box 2, filter 3, and reimaging lens 4 with the camera.
On the side of the reimaging lens we fix the unequal-arm interferometer with the screen. The camera is
not shown in the figure. In the front flange of the telescope and in the mount of the reimaging lens barrel,
we set diaphragms D1, D2 with a central aperture 1–2 mm. These apertures are reference for tracing of
the future optical axis of the telescope and for installation of teleobjective optics, field lens, BF,
reimaging lens, and CCD camera.
96
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
c
b
d
F
Figure 17. Wavvefront interferograms of the teleobjective: а is 1980, the first
f
assembly [[Klevtsov, 1987]; b is
2015 bbefore the disasssembly; c is thee assembly on M
May 5, 2015; d is the calculateed wavefront
F
Figure 18. Adjustment and co
ontrol scheme for the telesco
ope The numbeers at the top aare distances between
b
opticall elements, mm
m
97
Chromospheric telescope of Baikal Astrophysical Observatory. New light
The beam splitting cube of the interferometer is changed to a mirror prism for the adjustment period to get
rid of secondary reflection glares. By moving the interferometer, we direct a laser beam from the prism through
the aperture in the screen to the telescope and match it with the telescope axis through reference apertures of
the diaphragms.
The optical elements are set and adjusted according to their position in the optical scheme, starting
with the teleobjective.
The teleobjective. The teleobjective, assembled and adjusted in its barrel, is fixed in the front flange
of the telescope. By tilting the whole barrel, we adjust an interference image of reflection glares, which
reflected from surfaces of the teleobjective lenses, to the center of the interferometer screen.
The field lens is installed into its barrel. In this case it appeared that the optical center of the field
lens did not coincide with the center of the barrel. We had to turn the mount of the barrel and shift the
field lens along with the barrel by 1 mm to make the reflection glares reflected from its surface be within
the screen center.
BF. If the filter is set correctly, a laser beam should come to the center of the protective glass of the BF
optical stack and be reflected to the interferometer screen center. We gave surfaces of protective glasses in the
filter an anti-reflection coating for the red spectral region. To enhance brightness of the reflected laser beam,
we screwed a glass in barrel (mirror or cut filter) into a window flange of the filter. The surface of the glass had
been made parallel to the BF protective glass. Notice that the surface of the entrance IF should also be set
parallel to the entrance (exit) window of the crystal stack. BF is brought to the optical axis and to
autocollimation by longitudinal and inclined movements of a matching site. After the adjustment, BF is taken
out from the matching site because its passband does not transmit emission in the 6328 Å line. To control the
wavefront of the telescope in this line, we replace BF with a simulator made from a transparent glass.
The reimaging lens. The mount of the lens barrel with the installed base diaphragm D2 is
preliminarily set perpendicular to a laser beam, using autocollimation from an auxiliary mirror. The
objective lenses themselves and the lens barrel were well centered and after installation of the barrel
to the mount fell in the screen center.
The landing flange of the CCD camera (not shown in the figure) was adjusted to the axis of the
telescope, using a laser beam.
WAVEFRONT OF OPTICS OF THE CHROMOSPHERIC TELESCOPE
AND “NEW LIGHT”
Wavefront interferograms of the telescope (Figure 19) were obtained in the autocollimation scheme
with the reference flat mirror. Before exposure, optics had been «kept» for several hours to equalize
temperature gradients. The building where all the optical elements were located was blown by a fan.
98
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
b
c
d
e
f
F
Figure 19. Wavve aberrations of the Нα telescoope optics: calcculated wave ab
berrations (λ=0..6563 µm) for an
a axial
point ((a); those at thee edge of the fiield of view off 16 arcmin (b);; interferogramss (λ=0.6328 µm
m) in the doublle beam
path foor an axial poinnt, focal images (c, d); a postfoocal image (e); a prefocal imag
ge (f)
T
The interferoggrams show th
hat the qualityy of the telesccope optics en
nsures fulfillm
ment of the Raayleigh
criteriion. Wavefronnt distortions of
o the modernnized BF, whicch were meassured using seeparate blocks in the
Twym
man interferom
meter, are also within tolerabble limits. Belo
ow is given a full
f disk chrom
mospheric imaage and
scaledd-up fragmentss of the imagees captured in the Нα line ceenter and wing
g with an aperrture of 120 mm
m and
exposuure time of 0.0005 s in summeer 2015 (Figurres 20–24). The FWHM is 0.47 Å. Spatial rresolution is ~1.
G
Given the nom
minal diameter of the lenss of 170 mm
m and its high quality, it iss possible to obtain
higheer resolution images
i
underr good atmosppheric condittions; howeveer, the effectiive diameter of the
use a full-dissk image is taken
t
at reso
olution of thee telescope already
a
lens hhas been deccreased becau
determ
mined by mattrix and pixel sizes. The usse of the entirre aperture can
n lead to an inncrease in scaattered
light aand to an unjuustified increaase in the heaat load on BF.
IIn the telescoppe, by employ
ying the full aperture of 180 mm and the
t high-resollution cameraa under
good astroclimatic conditions, we
w can obtainn solar imagees with resolu
ution higher tthan 1′′ with image
w
0.05 Å across the fieeld of view.
monoochromaticity within
CONCL
LUSION
T
The chromosppheric telescop
pe of the Baikkal Astrophysiccal Observatorry is again reaady for observ
vations
withinn the solar patr
trol program an
nd for scientiffic research. We
W have made a new reimagging lens to taake full
solar ddisk images with
w the Hamam
matsu С9300-1124 digital cam
mera. All the telescope
t
opticcs have been cleaned
c
and reeadjusted. BF has been repaaired. Spectrall characteristiccs of the prefiilter and BF pprovide high-ccontrast
monocchromatic imaages. Wavefron
nt interferograams of optical elements and the
t telescope aas a whole sho
ow that
waveffront distortionns of the entire optical path arre within 0.25λλ.
99
Chromoospheric telescoppe of Baikal Astro
ophysical Observvatory. New light
O
Over a period from 1981 to 1999, 50 mm
m solar images were captured
d on an 80-mm
m film. The av
vailable
archivve of films haas many imagees with spatiall resolution off about 1. In 2000–2002, 550 mm imagees were
taken by the Princeton Instrumeents CCD cam
mera with a 50×50
5
mm maatrix detector,, 2048×2048 pixels.
Nowaadays, 18 mm solar images are captured bby the Hamam
matsu С9300-12
24 CCD cameera with a 36×2
24 mm
matrixx detector, 40000×2672 pixelss. There is slighhtly more than
n 1 pixel for 1″.
IIt is obvious that digital recording succcessfully com
mpetes againstt film recordiing, but this cannot
implyy an overwhelming advan
ntage of onee technology
y over anotheer [http://archhives.ru/documents/
methoodics/obzor_reestore-text-arcchival-documeent.shtml]. Resolution
R
off photomateriial depends on its
photoosensitivity. Prroper exposure and developpment time off a film can pro
ovide a higherr resolution im
mage if
the tellescope lens is not stopped down to 120 mm as we aree doing now to
o reduce useleess exposure. On the
other hand, even iff we set its diaaphragm to 12 0 mm, the exp
posure time of the CCD cam
mera for featu
ures on
the soolar disk is onne order of magnitude
m
shoorter than that of film recorrding; it is 5 ms with a dy
ynamic
range of around 4000. This is esssential for acqquisition of ten
ns and hundreeds of images less prone to seeing
effectts, for selection of the best images
i
or theiir post factum
m processing with
w regard to tthe flat field.
F
Figure 20. The chromosphere, the Hα line cennter, August 8, 2015, 09:01:00
0 LT
F
Figure 21. The chromosphere (a fragment of F
T
Figure 20), the Hα line center,, August 8, 201 5, 09:01:00 LT
100
V.I. Skoomorovsky, G.I. Kushtal,
K
L.S. Lopteva, V.A. Proshiin, V.D. Trifonov,, S.A. Chuprakov,, V.A. Khimich
F
Figure 22. The chromosphere, the +0.5 Å winng, August 8, 20
015, 09:06:01 LT
L
F
Figure 23. The chromosphere, the +0.2 Å winng, August 23, 2015,
2
15:21:18 LT
F
Figure 24. The chromosphere, the Hα line cennter, August 23, 2015, 17:13:17 LT
T
This is just thee digital techn
nology that faacilitates real-ttime registratiion and exchaange of solar images
i
in thee worldwide network of solar observattories. Addressses of the arrchive of the solar patrol of the
worlddwide networkk of solar staations and reeal-time Нα observations
o
are
a given on the website of the
101
Chromospheric telescope of Baikal Astrophysical Observatory. New light
National
Solar
Observatory
(the
USA)
[http://www.nso.edu/
IAU-Com12/resources,
http://www.hida.kyoto-u.ac.jp/ Smart/]. You can see that in the image quality the BAO chromospheric
telescope is highly competitive with telescopes of the worldwide network. Moreover, opportunity exists
to further increase its resolution by means of a higher resolution matrix.
We thank C.Sc. (Phys.&Math.) A.A. Golovko, A.A. Zhdanov not only for providing us with
solar observations to illustrate operation of the telescope but also for the image quality analysis
contributing to the modernization, as well as the head of the Baikal Astrophysical Observatory C.Sc.
(Phys.&Math.) A.V. Borovik – the main initiator and organizer of this great work – and the head of
the machining department V.S. Fedotov who supervised the fine adjustment of the telescope units
and the manufacture of technological devices for treating and controlling the telescope optics.
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